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<ri:Resource created="2026-01-23T19:39:37Z" status="active" updated="2026-03-02T06:25:50Z" version="1.2" xmlns:cs="http://www.ivoa.net/xml/ConeSearch/v1.0" xmlns:ri="http://www.ivoa.net/xml/RegistryInterface/v1.0" xmlns:vr="http://www.ivoa.net/xml/VOResource/v1.0" xmlns:vs="http://www.ivoa.net/xml/VODataService/v1.1" xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance" xsi:schemaLocation="http://www.ivoa.net/xml/ConeSearch/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/ConeSearch.xsd http://www.ivoa.net/xml/VOResource/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/VOResource.xsd http://www.ivoa.net/xml/VODataService/v1.1 http://vo.ari.uni-heidelberg.de/docs/schemata/VODataService.xsd" xsi:type="vs:CatalogService"><title>5 oscillating eclipsing Algols puls. frequencies</title><shortName>J/A+A/705/A251</shortName><identifier>ivo://CDS.VizieR/J/A+A/705/A251</identifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Pawar T.</name></creator><creator><name>Miszuda A.</name></creator><creator><name>Helminiak K.G.</name></creator><creator><name>Marcadon F.</name></creator><creator><name>Moharana A.</name></creator><creator><name>Pawar G.,Konacki M.</name></creator><date role="Updated">2026-03-02T06:25:50Z</date><date role="Created">2026-01-23T19:39:37Z</date><contact><name>CDS support team</name><address>CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France</address><email>cds-question@unistra.fr</email></contact></curation><content><subject>eclipsing-binary-stars</subject><subject>asteroseismology</subject><subject>visible-astronomy</subject><description>Eclipsing double-lined spectroscopic binaries (SB2s) hosting delta Scuti-type pulsators offer a unique laboratory for simultaneously constraining stellar geometry and interior structure. In this study, we present a comprehensive analysis of five oscillating eclipsing Algol (oEA) binaries. By combining high-precision, short-cadence TESS photometry with multi-epoch high-resolution spectroscopy, we derive precise stellar and orbital parameters. Frequency power spectra were obtained using residuals from binary modelling. We further investigate the evolutionary history of these systems using a grid of MESA binary evolution simulations. Our analysis suggests that the systems must have undergone either case A or case B mass transfer, with the primary components repositioned in the Hertzsprung-Russell diagram and now pulsating in the delta Scuti regime, while the cooler secondaries are underluminous and inflated, filling their Roche lobes. 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